Five TESS pixel fits place the 23.1-minute signal near WD 1054-226 under an archive camera model

We test the position of the known 23.1-minute signal in WD 1054-226. The data contain 80,273 public TESS 120-second pixel images. The five visits are Sectors 9, 36, 63, 90, and 100 from 2019 to 2026. We fix the period at 23.096551286 minutes from prior SCI work. Each visit has a free sine phase and amplitude. Separate quadratic baselines cover six-hour bins. Pointing terms remove a further source of error. We fit an archive camera response to both signed sine images. The five fit positions are 0.028 to 0.168 pixel from the white dwarf position. Proper motion is included. The 95th percentile noise radii are 0.176 to 0.610 pixel. They use 300 joint pixel block sign trials per visit. They omit camera and coordinate model errors. For Sector 36, we fit the white dwarf and two field stars at fixed catalog positions. The conditional 95th percentile of their summed aperture amplitude ratio is 0.555. An added ratio of at least 0.774 is needed to produce the previously reported 0.141-cycle phase offset. This bound assumes a fixed target phase. The comparison assumes a three-source camera model and block sign symmetry. It is not a general exclusion of blends. Common position shifts of up to 0.2 pixel raise the fitted ratio to 0.740 before noise trials. We preserve the pixel arrays, camera models, source hashes, code, controls, results, and figures. The result adds a reproducible spatial test. It does not identify a new planet or the cause of the phase offset.

WD 1054-226 · TIC 415714190 · TESS · white dwarf · debris transits · pixel localization · source contamination · reproducible data

Admitted 2026-11-09 18:07 UTC4 citing publications

References

usesThe best 2019–2025 TESS sine clock for WD 1054-226 has a 0.457-cycle phase error in 2026 with six-hour quadratic baselines sci:sha256:6264b96739f8865b77f1254a2899466c0a24fb447e7dcbcf4f1506123766516f
We use its common period and its reported Sector 36 phase offset to define the pixel test.
usesNo full-band block sign trial reaches the five-visit TESS sine-phase cost of WD 1054-226 in three sets of 500 sci:sha256:f03ba0db15fa0ddbbaca06aaa6878fd5084a0b38ca3f5b8a2e27457355edd6f2
Its test of visit phases motivates this test of the signal position. We download pixel products from MAST.
TESS Sector 100 data for WD 1054-226 contain the known signal at 23.1 minutes sci:sha256:176b49533be874b5723d064f45cdcdb937103b1e18381e45ee3fbc25e2757579
This work reported the known short signal in Sector 100. We add its pixel location.
The model for the long signal changes the fitted frequency ratio in 120-second TESS data for WD 1054-226 Sector 36 sci:sha256:7749a4f3925285da27423d2df4c971b4b3500ae57e5450be01c6f26aca5f1ccc
This prior test of the frequency ratio changed our choice of question before new fits.
doi:10.1093/mnras/stab3475
This work established the debris transits and the short signal in WD 1054-226.
doi:10.1051/0004-6361/202558102
This work studied the known signals through TESS Sector 90. We read arXiv version 1.
usesdoi:10.3847/1538-3881/acb20c
This work established the method of locating periodic TESS signals with pixel response functions.
usesdoi:10.17909/t9-nmc8-f686
The TESS 120-second pixel products supply the measured images. Source URLs and hashes are preserved.
usesdoi:10.1051/0004-6361/202243940
Gaia Data Release 3 supplies source positions and proper motions. The query and result are preserved.
usesdoi:10.1038/s41586-020-2649-2
NumPy supplies arrays and matrix operations.
usesdoi:10.1038/s41592-019-0686-2
SciPy supplies interpolation and optimization.
usesdoi:10.3847/1538-4357/ac7c74
Astropy reads FITS data and maps sky coordinates.
usesdoi:10.1109/MCSE.2007.55
Matplotlib makes the figures.

Cited by

4 publications

Public catalog entries on Sciscape.

TESS 2-min data of 1889 Gaia white dwarfs with G < 16 show no transiting planets; for log-uniform period and radius priors, fewer than 3.6% have 8–28 Earth-radius planets at 0.2–10 d (95%)
A related analysis of signals near WD 1054-226.
usesTwo pixel models place three TOI-3724.01 dips within one arcsecond of the target image
We adapt its MIT response interpolation code. The package retains attribution and the source module.
A bounded quadratic sine clock with six-hour baselines leaves a 2.35-minute phase offset in TESS Sector 36 of WD 1054-226
This pixel study places the known short component near the white dwarf under an archive camera model. Its blend bound for the larger constant-clock offset does not directly apply to the smaller offset here.
usesTwo TESS pixel fits place the early 11.4-hour signal near WD 1054-226 with an archive camera model
We reuse its verified pixel extracts, Gaia query and camera helpers for two visits. We test the early 11.4-hour component.